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A finite-size particle scheme for the numerical solution of twoand three-dimensional gasdynamic problems of astronomical interest is described and tested. The scheme is then applied to the fission problem for optically thick protostars. Results are given, showing the evolution of one such protostar from an initial state as a single rotating star to a final state as a triple system whose components contain 60% of the original mass. The decisiveness of this numerical test of the fission hypothesis and its relevance to observed binaries are briefly discussed.
L. B. Lucy (Thu,) studied this question.
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